Large scale primordial magnetic fields from inflation and preheating

Physics

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Large scale primordial magnetic fields from inflation and preheating. / Tornkvist, Ola; Davis, Anne-Christine; Dimopoulos, Konstantinos et al.
COSMOLOGY AND PARTICLE PHYSICS: CAPP 2000: Proceedings. ed. / Ruth Durrer; Juan Garcia- Bellido; Mikhail Shaposhnikov. Melville, N.Y.: American Institute of Physics, 2000. p. 443-446.

Research output: Contribution in Book/Report/Proceedings - With ISBN/ISSN › Chapter

Harvard

Tornkvist, O, Davis, A-C, Dimopoulos, K & Prokopec, T 2000, Large scale primordial magnetic fields from inflation and preheating. in R Durrer, J Garcia- Bellido & M Shaposhnikov (eds), COSMOLOGY AND PARTICLE PHYSICS: CAPP 2000: Proceedings. American Institute of Physics, Melville, N.Y., pp. 443-446.

APA

Tornkvist, O., Davis, A.-C., Dimopoulos, K., & Prokopec, T. (2000). Large scale primordial magnetic fields from inflation and preheating. In R. Durrer, J. Garcia- Bellido, & M. Shaposhnikov (Eds.), COSMOLOGY AND PARTICLE PHYSICS: CAPP 2000: Proceedings (pp. 443-446). American Institute of Physics.

Vancouver

Tornkvist O, Davis AC, Dimopoulos K, Prokopec T. Large scale primordial magnetic fields from inflation and preheating. In Durrer R, Garcia- Bellido J, Shaposhnikov M, editors, COSMOLOGY AND PARTICLE PHYSICS: CAPP 2000: Proceedings. Melville, N.Y.: American Institute of Physics. 2000. p. 443-446

Author

Tornkvist, Ola ; Davis, Anne-Christine ; Dimopoulos, Konstantinos et al. / Large scale primordial magnetic fields from inflation and preheating. COSMOLOGY AND PARTICLE PHYSICS: CAPP 2000: Proceedings. editor / Ruth Durrer ; Juan Garcia- Bellido ; Mikhail Shaposhnikov. Melville, N.Y. : American Institute of Physics, 2000. pp. 443-446

Bibtex

@inbook{a164ea90f933449b9b465eac060c4b3c,

title = "Large scale primordial magnetic fields from inflation and preheating",

abstract = "We consider models in which the (transverse) photon mass is non-zero during inflation and drops to zero non-adiabatically at the end of inflation. Through this process, vacuum fluctuations of the photon field are converted into physical, long-wavelength modes with high amplitude. The resulting spectrum of the field strength is approximately B_l ~ 1/l, where l is the relevant coherence scale. With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields.",

author = "Ola Tornkvist and Anne-Christine Davis and Konstantinos Dimopoulos and Tomislav Prokopec",

year = "2000",

language = "English",

pages = "443--446",

editor = "Ruth Durrer and {Garcia- Bellido}, Juan and Mikhail Shaposhnikov",

booktitle = "COSMOLOGY AND PARTICLE PHYSICS: CAPP 2000: Proceedings",

publisher = "American Institute of Physics",

}

RIS

TY - CHAP

T1 - Large scale primordial magnetic fields from inflation and preheating

AU - Tornkvist, Ola

AU - Davis, Anne-Christine

AU - Dimopoulos, Konstantinos

AU - Prokopec, Tomislav

PY - 2000

Y1 - 2000

N2 - We consider models in which the (transverse) photon mass is non-zero during inflation and drops to zero non-adiabatically at the end of inflation. Through this process, vacuum fluctuations of the photon field are converted into physical, long-wavelength modes with high amplitude. The resulting spectrum of the field strength is approximately B_l ~ 1/l, where l is the relevant coherence scale. With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields.

AB - We consider models in which the (transverse) photon mass is non-zero during inflation and drops to zero non-adiabatically at the end of inflation. Through this process, vacuum fluctuations of the photon field are converted into physical, long-wavelength modes with high amplitude. The resulting spectrum of the field strength is approximately B_l ~ 1/l, where l is the relevant coherence scale. With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields.

M3 - Chapter

SP - 443

EP - 446

BT - COSMOLOGY AND PARTICLE PHYSICS: CAPP 2000: Proceedings

A2 - Durrer, Ruth

A2 - Garcia- Bellido, Juan

A2 - Shaposhnikov, Mikhail

PB - American Institute of Physics

CY - Melville, N.Y.

ER -

Research

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